Diffusion of magnetic fields relative to plasma as a result of turbulent reconnection is termed as “reconnection diffusion (RD)"
[1]}, [2]}, [3]}.
It has been applied in the context of star formation and well explains observations
(e.g.,[4]}, [5]}, [6]}).
Despite its importance, RD was disregarded in earlier studies of nonlinear turbulent dynamo.
We stress that although some microphysical effects, e.g., ambipolar diffusion,
were discussed in the literature as nonlinear effects
[7]}, [8]},
the “nonlinear" dynamo considered here is characterized by the energy equipartition between turbulence and magnetic fields
and by the development of MHD turbulence because of the dynamical effect of magnetic fields on turbulence.
